Li data (LTE) for our solar-metallicity subsample (−0.2 ≤ [Fe/H] ≤ +0.2; circles and triangles: Li determinations and upper limits) as a function of effective temperature as proxy for evolution (from high to cool values). Tracks show the predictions for Li behaviour as the stars evolve from the subgiant branch to the RGB tip and later from the clump to AGB phase from the non-rotating models with thermohaline mixing (solid) and the models including rotation and thermohaline mixing (others) from Lagarde et al. (2012) computed for [Fe/H] = 0. At this metallicity, the initial Li abundance assumed in the models is 3.11 dex. In the left and right panels we plot respectively the stars with masses ≤ and > 2 M_⊙. The initial masses of the models are colour-labeled, with information on the initial (ZAMS) rotation velocity.